Epoch J2000.0 Equinox J2000.0 (ICRS)
|Right ascension||06h 45m 08.9173s[note 1]|
|Declination||−16° 42′ 58.017″[note 1]|
|Apparent magnitude (V)||−1.47 (A) / 8.30 (B)|
|Spectral type||A1V (A) / DA2 (B)|
|U−B color index||−0.05 (A) / −1.04 (B)|
|B−V color index||0.01 (A) / −0.03 (B)|
|Radial velocity (Rv)||−7.6 km/s|
|Proper motion (μ)||RA: −546.05[note 1] mas/yr
Dec.: −1223.14[note 1] mas/yr
|Parallax (π)||379.21 ± 1.58 mas|
|Distance||8.60 ± 0.04 ly
(2.64 ± 0.01 pc)
|Absolute magnitude (MV)||1.42 (A)[note 2] / 11.18 (B)|
|Companion||α CMa B|
|Period (P)||50.090 ± 0.055 yr|
|Semi-major axis (a)||7.50 ± 0.04"|
|Eccentricity (e)||0.5923 ± 0.0019|
|Inclination (i)||136.53 ± 0.43°|
|Longitude of the node (Ω)||44.57 ± 0.44°|
|Periastron epoch (T)||1894.130 ± 0.015|
|Argument of periastron (ω)
|147.27 ± 0.54°|
|α CMa A|
|Surface gravity (log g)||4.33 cgs|
|Metallicity [Fe/H]||0.50 dex|
|Age||2–3 × 108 years|
|α CMa B|
|Radius||0.0084 ± 3% R☉|
|Luminosity||0.026[note 3] L☉|
|Surface gravity (log g)||8.57 cgs|
Sirius (//) is the brightest star (in fact, a star system) in the Earth's night sky. With a visual apparent magnitude of −1.46, it is almost twice as bright as Canopus, the next brightest star. The name "Sirius" is derived from the Ancient Greek: Σείριος Seirios ("glowing" or "scorcher"). The system has the Bayer designation Alpha Canis Majoris (α CMa). What the naked eye perceives as a single star is actually a binary star system, consisting of a white main-sequence star of spectral type A1V, termed Sirius A, and a faint white dwarf companion of spectral type DA2, called Sirius B. The distance separating Sirius A from its companion varies between 8.2 and 31.5 AU.
Sirius appears bright because of both its intrinsic luminosity and its proximity to Earth. At a distance of 2.6 parsecs (8.6 ly), as determined by the Hipparcos astrometry satellite, the Sirius system is one of Earth's near neighbors. Sirius is gradually moving closer to the Solar System, so it will slightly increase in brightness over the next 60,000 years. After that time its distance will begin to recede, but it will continue to be the brightest star in the Earth's sky for the next 210,000 years.
Sirius A is about twice as massive as the Sun (M☉) and has an absolute visual magnitude of 1.42. It is 25 times more luminous than the Sun but has a significantly lower luminosity than other bright stars such as Canopus or Rigel. The system is between 200 and 300 million years old. It was originally composed of two bright bluish stars. The more massive of these, Sirius B, consumed its resources and became a red giant before shedding its outer layers and collapsing into its current state as a white dwarf around 120 million years ago.
Sirius is also known colloquially as the "Dog Star", reflecting its prominence in its constellation, Canis Major (Greater Dog). The heliacal rising of Sirius marked the flooding of the Nile in Ancient Egypt and the "dog days" of summer for the ancient Greeks, while to the Polynesians in the southern hemisphere it marked winter and was an important star for navigation around the Pacific Ocean.
- 1 Observational history
- 2 Visibility
- 3 System
- 4 Etymology and cultural significance
- 5 See also
- 6 Notes
- 7 References
- 8 External links
Sirius, known in ancient Egypt as Sopdet (Greek: Σῶθις Sothis), is recorded in the earliest astronomical records. During the era of the Middle Kingdom, Egyptians based their calendar on the heliacal rising of Sirius, namely the day it becomes visible just before sunrise after moving far enough away from the glare of the Sun. This occurred just before the annual flooding of the Nile and the summer solstice, after a 70-day absence from the skies. The hieroglyph for Sothis features a star and a triangle. Sothis was identified with the great goddess Isis, who formed a part of a triad with her husband Osiris and their son Horus, while the 70-day period symbolised the passing of Isis and Osiris through the duat (Egyptian underworld).
The ancient Greeks observed that the appearance of Sirius heralded the hot and dry summer, and feared that it caused plants to wilt, men to weaken, and women to become aroused. Due to its brightness, Sirius would have been noted to twinkle more in the unsettled weather conditions of early summer. To Greek observers, this signified certain emanations which caused its malignant influence. Anyone suffering its effects was said to be astroboletos (ἀστροβόλητος) or "star-struck". It was described as "burning" or "flaming" in literature. The season following the star's heliacal rising (i.e. rising with the Sun) came to be known as the Dog Days of summer. The inhabitants of the island of Ceos in the Aegean Sea would offer sacrifices to Sirius and Zeus to bring cooling breezes, and would await the reappearance of the star in summer. If it rose clear, it would portend good fortune; if it was misty or faint then it foretold (or emanated) pestilence. Coins retrieved from the island from the 3rd century BC feature dogs or stars with emanating rays, highlighting Sirius' importance. The Romans celebrated the heliacal setting of Sirius around April 25, sacrificing a dog, along with incense, wine, and a sheep, to the goddess Robigo so that the star's emanations would not cause wheat rust on wheat crops that year.
Ptolemy of Alexandria mapped the stars in Books VII and VIII of his Almagest, in which he used Sirius as the location for the globe's central meridian. He curiously depicted it as one of six red-coloured stars (see the Red controversy section below). The other five are class M and K stars, such as Arcturus and Betelgeuse.
Bright stars were important to the ancient Polynesians for navigation between the many islands and atolls of the Pacific Ocean. Low on the horizon, they acted as stellar compasses to assist mariners in charting courses to particular destinations. They also served as latitude markers; the declination of Sirius matches the latitude of the archipelago of Fiji at 17°S and thus passes directly over the islands each night. Sirius served as the body of a "Great Bird" constellation called Manu, with Canopus as the southern wingtip and Procyon the northern wingtip, which divided the Polynesian night sky into two hemispheres. Just as the appearance of Sirius in the morning sky marked summer in Greece, so it marked the chilly onset of winter for the Māori, whose name Takurua described both the star and the season. Its culmination at the winter solstice was marked by celebration in Hawaii, where it was known as Ka'ulua, "Queen of Heaven". Many other Polynesian names have been recorded, including Tau-ua in the Marquesas Islands, Rehua in New Zealand, and Ta'urua-fau-papa "Festivity of original high chiefs" and Ta'urua-e-hiti-i-te-tara-te-feiai "Festivity who rises with prayers and religious ceremonies" in Tahiti. The Hawaiian people had many names for Sirius, including Aa ("glowing"), Hoku-kauopae, Kau-ano-meha (also Kaulanomeha), "Standing-alone-and-sacred", Hiki-kauelia or Hiki-kauilia (the navigational name), Hiki-kau-lono-meha ("star of solitary Lono", the astrological name), Kaulua (also Kaulua-ihai-mohai, "flower of the heavens"), Hiki-kauelia, Hoku-hoo-kele-waa ("star which causes the canoe to sail", a marine navigation name), and Kaulua-lena ("yellow star"). The people of the Society Islands called Sirius variously Taurua-fau-papa, Taurua-nui-te-amo-aha, and Taurua-e-hiti-i-tara-te-feiai. Other names for Sirius included Palolo-mua (Futuna), Mere (Mangaia), Apura (Manihiki), Taku-ua (Marquesas Islands), and Tokiva (Pukapuka). In the cosmology of the Tuamotus, Sirius had various names, including Takurua-te-upuupu, Te Kaha ("coconut fiber"), Te Upuupu, Taranga, and Vero-ma-torutoru ("flaming and diminishing").
In 1718, Edmond Halley discovered the proper motion of the hitherto presumed "fixed" stars after comparing contemporary astrometric measurements with those given in Ptolemy's Almagest. The bright stars Aldebaran, Arcturus and Sirius were noted to have moved significantly, the last of which having progressed 30 arc minutes (about the diameter of the Moon) southwards in 1,800 years.
In 1868, Sirius became the first star to have its velocity measured. Sir William Huggins examined the spectrum of this star and observed a noticeable red shift. He concluded that Sirius was receding from the Solar System at about 40 km/s. Compared to the modern value of −7.6 km/s, this both was an overestimate and had the wrong sign; the minus means it is approaching the Sun. However, it is notable for introducing the study of celestial radial velocities.
The parallax of Sirius was measured by Thomas Henderson using his observations made in 1832-1833 and Maclear's observations made in 1836-1837, and was published in 1839. The value of the parallax was 0.23 arcseconds, and error of the parallax was estimated not to exceed a quarter of a second.
Also, were earlier attempts to measure parallax of Sirius: by the second Cassini (6 seconds); by some astronomers (including Nevil Maskelyne) using Lacaille's observations made at the Cape of Good Hope (4 seconds); by Piazzi (the same amount); using Lacaille's observations made at Paris, more numerous and certain than those made at the Cape (no sensible parallax); by Bessel (no sensible parallax).
Sirius distance estimates
|Source||Parallax, mas||Distance, pc||Distance, ly||Distance, Pm||Ref.|
|Henderson (1840)||~ 230||~ 4.3||~ 14.2||~ 134.2|||
|Woolley et al. (1970)||377±4||2.653±0.028||8.65±0.09||81.8±0.9|||
|Gliese & Jahreiß (1991)||380.4±2.9||2.629±0.02||8.57+0.07
|van Altena et al. (1995)||381.6±2.2||2.621±0.015||8.55±0.05||80.9±0.5|||
|Perryman et al. (1997) (Hipparcos)||379.21±1.58||2.637±0.011||8.6±0.04||81.4±0.3|||
|Perryman et al. (1997) (Tycho)||(absents)|||
|van Leeuwen (2007)||379.21±1.58[note 4]||2.637±0.011||8.6±0.04||81.4±0.3|||
|RECONS TOP100 (2012)||380.02±1.28[note 5]||2.631±0.009||8.583±0.029||81.2±0.27|||
Non-trigonometric distance estimates are marked in italic. The most precise estimate is marked in bold.
Discovery of a companion
In 1844 the German astronomer Friedrich Bessel deduced from changes in the proper motion of Sirius that it had an unseen companion. Nearly two decades later, on January 31, 1862, American telescope-maker and astronomer Alvan Graham Clark first observed the faint companion, which is now called Sirius B, or affectionately "the Pup". This happened during testing of an 18.5-inch (470 mm) aperture great refractor telescope for Dearborn Observatory, which was the largest refracting telescope lens in existence at the time, and the largest telescope in the United States. Sirius B sighting was confirmed on March 8 with smaller telescopes as well.
The visible star is now sometimes known as Sirius A. Since 1894, some apparent orbital irregularities in the Sirius system have been observed, suggesting a third very small companion star, but this has never been definitely confirmed. The best fit to the data indicates a six-year orbit around Sirius A and a mass of only 0.06 M☉. This star would be five to ten magnitudes fainter than the white dwarf Sirius B, which would account for the difficulty of observing it. Observations published in 2008 were unable to detect either a third star or a planet. An apparent "third star" observed in the 1920s is now confirmed as a background object.
In 1915, Walter Sydney Adams, using a 60-inch (1.5 m) reflector at Mount Wilson Observatory, observed the spectrum of Sirius B and determined that it was a faint whitish star. This led astronomers to conclude that it was a white dwarf, the second to be discovered. The diameter of Sirius A was first measured by Robert Hanbury Brown and Richard Q. Twiss in 1959 at Jodrell Bank using their stellar intensity interferometer. In 2005, using the Hubble Space Telescope, astronomers determined that Sirius B has nearly the diameter of the Earth, 12,000 kilometers (7,500 mi), with a mass that is 98% of the Sun.
Around 150 AD, the Greek astronomer of the Roman period Claudius Ptolemy described Sirius as reddish, along with five other stars, Betelgeuse, Antares, Aldebaran, Arcturus and Pollux, all of which are clearly of orange or red hue. The discrepancy was first noted by amateur astronomer Thomas Barker, squire of Lyndon Hall in Rutland, who prepared a paper and spoke at a meeting of the Royal Society in London in 1760. The existence of other stars changing in brightness gave credence to the idea that some may change in color too; Sir John Herschel noted this in 1839, possibly influenced by witnessing Eta Carinae two years earlier. Thomas Jefferson Jackson See resurrected discussion on red Sirius with the publication of several papers in 1892, and a final summary in 1926. He cited not only Ptolemy but also the poet Aratus, the orator Cicero, and general Germanicus as coloring the star red, though acknowledging that none of the latter three authors were astronomers, the last two merely translating Aratus' poem Phaenomena. Seneca, too, had described Sirius as being of a deeper red color than Mars. However, not all ancient observers saw Sirius as red. The 1st century AD poet Marcus Manilius described it as "sea-blue", as did the 4th century Avienus. It is the standard star for the color white in ancient China, and multiple records from the 2nd century BC up to the 7th century AD all describe Sirius as white in hue.
In 1985, German astronomers Wolfhard Schlosser and Werner Bergmann published an account of an 8th-century Lombardic manuscript, which contains De cursu stellarum ratio by St. Gregory of Tours. The Latin text taught readers how to determine the times of nighttime prayers from positions of the stars, and Sirius is described within as rubeola — "reddish". The authors proposed this was further evidence Sirius B had been a red giant at the time. However, other scholars replied that it was likely St. Gregory had been referring to Arcturus instead.
The possibility that stellar evolution of either Sirius A or Sirius B could be responsible for this discrepancy has been rejected by astronomers on the grounds that the timescale of thousands of years is too short and that there is no sign of the nebulosity in the system that would be expected had such a change taken place. An interaction with a third star, to date undiscovered, has also been proposed as a possibility for a red appearance. Alternative explanations are either that the description as red is a poetic metaphor for ill fortune, or that the dramatic scintillations of the star when it was observed rising left the viewer with the impression that it was red. To the naked eye, it often appears to be flashing with red, white and blue hues when near the horizon.
With an apparent magnitude of −1.46, Sirius is the brightest star system in the night sky, almost twice the brightness of the second brightest star, Canopus. However, it is not as bright as the Moon, Venus, or Jupiter, and at times, Mercury and Mars are also brighter than Sirius. Sirius can be seen from almost everywhere on the Earth's surface, with only observers north of 73 degrees latitude unable to see it, and it does not rise very high when viewed from some northern cities, reaching only 13° above the horizon from Saint Petersburg. Sirius, along with Procyon and Betelgeuse, forms one of the three vertices of the Winter Triangle to observers in the Northern Hemisphere. Due to its declination of roughly −17°, Sirius is a circumpolar star from latitudes south of 73° S. From the Southern Hemisphere in early July, Sirius can be seen in both the evening where it sets after the Sun, and in the morning where it rises before the Sun. Due to precession (and slight proper motion), Sirius will move further south in the future. Starting in the year 9000, Sirius will not be visible any more from northern and central Europe, and in 14000 its declination will be -67° and thus it will be circumpolar throughout South Africa and in most parts of Australia.
Sirius can even be observed in daylight with the naked eye under the right conditions. Ideally, the sky should be very clear, with the observer at a high altitude, the star passing overhead, and the Sun low down on the horizon. These observing conditions are more easily met in the southern hemisphere, due to the southerly declination of Sirius.
The orbital motion of the Sirius binary system brings the two stars to a minimum angular separation of 3 arcseconds and a maximum of 11 arcseconds. At the closest approach, it is an observational challenge to distinguish the white dwarf from its more luminous companion, requiring a telescope with at least 300 mm (12 in) aperture and excellent seeing conditions. A periastron occurred in 1994[note 6] and the pair have since been moving apart, making them easier to separate with a telescope.
At a distance of 2.6 parsecs (8.6 ly), the Sirius system contains two of the eight nearest stars to the Solar System (not including the Sun), and is the fifth closest stellar system to ours (again not including the Sun). This proximity is the main reason for its brightness, as with other near stars such as Alpha Centauri and in stark contrast to distant, highly luminous supergiants such as Canopus, Rigel or Betelgeuse. However, it is still around 25 times more luminous than the Sun. The closest large neighbouring star to Sirius is Procyon, 1.61 parsecs (5.24 ly) away. The Voyager 2 spacecraft, launched in 1977 to study the four Jovian planets in the Solar System, is expected to pass within 4.3 light-years (1.3 pc) of Sirius in approximately 296,000 years.
Sirius is a binary star system consisting of two white stars orbiting each other with a separation of about 20 astronomical units (3.0×109 km; 1.9×109 mi)[note 7] (roughly the distance between the Sun and Uranus) and a period of 50.1 years. The brighter component, termed Sirius A, is a main-sequence star of spectral type A1V, with an estimated surface temperature of 9,940 K. Its companion, Sirius B, is a star that has already evolved off the main sequence and become a white dwarf. Currently 10,000 times less luminous in the visual spectrum, Sirius B was once the more massive of the two. The age of the system has been estimated at around 230 million years. Early in its lifespan it was thought to have been two bluish white stars orbiting each other in an elliptical orbit every 9.1 years. The system emits a higher than expected level of infrared radiation, as measured by IRAS space-based observatory. This may be an indication of dust in the system, and is considered somewhat unusual for a binary star. The Chandra X-ray Observatory image shows Sirius B outshining its bright partner as it is a brighter X-ray source.
Sirius A has a mass of 2 M☉. The radius of this star has been measured by an astronomical interferometer, giving an estimated angular diameter of 5.936±0.016 mas. The projected rotational velocity is a relatively low 16 km/s, which does not produce any significant flattening of its disk. This is at marked variance with the similar-sized Vega, which rotates at a much faster 274 km/s and bulges prominently around its equator. A weak magnetic field has been detected on the surface of Sirius A.
Stellar models suggest that the star formed during the collapsing of a molecular cloud, and that after 10 million years, its internal energy generation was derived entirely from nuclear reactions. The core became convective and utilized the CNO cycle for energy generation. It is predicted that Sirius A will have completely exhausted the store of hydrogen at its core within a billion (109) years of its formation. At this point it will pass through a red giant stage, then settle down to become a white dwarf.
Sirius A is classed as an Am star because the spectrum shows deep metallic absorption lines, indicating an enhancement in elements heavier than helium, such as iron. When compared to the Sun, the proportion of iron in the atmosphere of Sirius A relative to hydrogen is given by , which is equivalent to 100.5, meaning it has 316% of the proportion of iron in the Sun's atmosphere. The high surface content of metallic elements is unlikely to be true of the entire star, rather the iron-peak and heavy metals are radiatively levitated towards the surface.
With a mass nearly equal to the Sun's, Sirius B is one of the more massive white dwarfs known (0.98 M☉); it is almost double the 0.5–0.6 M☉ average. Yet that same mass is packed into a volume roughly equal to the Earth's. The current surface temperature is 25,200 K. However, because there is no internal heat source, Sirius B will steadily cool as the remaining heat is radiated into space over a period of more than two billion years.
A white dwarf forms only after the star has evolved from the main sequence and then passed through a red-giant stage. This occurred when Sirius B was less than half its current age, around 120 million years ago. The original star had an estimated 5 M☉ and was a B-type star (roughly B4–5) when it still was on the main sequence. While it passed through the red giant stage, Sirius B may have enriched the metallicity of its companion.
This star is primarily composed of a carbon–oxygen mixture that was generated by helium fusion in the progenitor star. This is overlaid by an envelope of lighter elements, with the materials segregated by mass because of the high surface gravity. Hence the outer atmosphere of Sirius B is now almost pure hydrogen—the element with the lowest mass—and no other elements are seen in its spectrum.
Sirius star cluster
In 1909, Ejnar Hertzsprung was the first to suggest that Sirius was a member of the Ursa Major Moving Group, based on his observations of the system's movements across the sky. The Ursa Major Group is a set of 220 stars that share a common motion through space and were once formed as members of an open cluster, which has since become gravitationally unbound. However, analyses in 2003 and 2005 found Sirius's membership in the group to be questionable: the Ursa Major Group has an estimated age of 500±100 million years, whereas Sirius, with metallicity similar to the Sun's, has an age that is only half this, making it too young to belong to the group. Sirius may instead be a member of the proposed Sirius Supercluster, along with other scattered stars such as Beta Aurigae, Alpha Coronae Borealis, Beta Crateris, Beta Eridani and Beta Serpentis. This is one of three large clusters located within 500 light-years (150 pc) of the Sun. The other two are the Hyades and the Pleiades, and each of these clusters consists of hundreds of stars.
Etymology and cultural significance
The most commonly used proper name of this star comes from the Latin Sīrius, from the Ancient Greek Σείριος (Seirios, "glowing" or "scorcher"), although the Greek word itself may have been imported from elsewhere before the Archaic period, one authority suggesting a link with the Egyptian god Osiris. The name's earliest recorded use dates from the 7th century BC in Hesiod's poetic work Works and Days. Sirius has over 50 other designations and names attached to it. In Geoffrey Chaucer's essay Treatise on the Astrolabe, it bears the name Alhabor, and is depicted by a hound's head. This name is widely used on medieval astrolabes from Western Europe. In Sanskrit it is known as Mrgavyadha "deer hunter", or Lubdhaka "hunter". As Mrgavyadha, the star represents Rudra (Shiva). The star is referred as Makarajyoti in Malayalam and has religious significance to the pilgrim center Sabarimala. In Scandinavia, the star has been known as Lokabrenna ("burning done by Loki", or "Loki's torch"). In the astrology of the Middle Ages, Sirius was a Behenian fixed star, associated with beryl and juniper. Its astrological symbol was listed by Heinrich Cornelius Agrippa.
Many cultures have historically attached special significance to Sirius, particularly in relation to dogs. Indeed, it is often colloquially called the "Dog Star" as the brightest star of Canis Major, the "Great Dog" constellation.
It was classically depicted as Orion's dog. The Ancient Greeks thought that Sirius's emanations could affect dogs adversely, making them behave abnormally during the "dog days," the hottest days of the summer. The Romans knew these days as dies caniculares, and the star Sirius was called Canicula, "little dog." The excessive panting of dogs in hot weather was thought to place them at risk of desiccation and disease. In extreme cases, a foaming dog might have rabies, which could infect and kill humans whom they had bitten. Homer, in the Iliad, describes the approach of Achilles toward Troy in these words:
Sirius rises late in the dark, liquid sky
On summer nights, star of stars,
Orion's Dog they call it, brightest
Of all, but an evil portent, bringing heat
And fevers to suffering humanity.
In Iranian mythology, especially in Persian mythology and in Zoroastrianism, the ancient religion of Persia, Sirius appears as Tishtrya and is revered as the rain-maker divinity (Tishtar of New Persian poetry). Beside passages in the sacred texts of the Avesta, the Avestan language Tishtrya followed by the version Tir in Middle and New Persian is also depicted in the Persian epic Shahnameh of Ferdowsi. Due to the concept of the yazatas, powers which are "worthy of worship", Tishtrya is a divinity of rain and fertility and an antagonist of apaosha, the demon of drought. In this struggle, Tishtrya is beautifully depicted as a white horse.
In Chinese astronomy the star is known as the star of the "celestial wolf" (Chinese and Japanese: 天狼 Chinese romanization: Tiānláng; Japanese romanization: Tenrō;) in the Mansion of Jǐng (井宿). Farther afield, many nations among the indigenous peoples of North America also associated Sirius with canines; the Seri and Tohono O'odham of the southwest note the star as a dog that follows mountain sheep, while the Blackfoot called it "Dog-face". The Cherokee paired Sirius with Antares as a dog-star guardian of either end of the "Path of Souls". The Pawnee of Nebraska had several associations; the Wolf (Skidi) tribe knew it as the "Wolf Star", while other branches knew it as the "Coyote Star". Further north, the Alaskan Inuit of the Bering Strait called it "Moon Dog".
Several cultures also associated the star with a bow and arrows. The Ancient Chinese visualized a large bow and arrow across the southern sky, formed by the constellations of Puppis and Canis Major. In this, the arrow tip is pointed at the wolf Sirius. A similar association is depicted at the Temple of Hathor in Dendera, where the goddess Satet has drawn her arrow at Hathor (Sirius). Known as "Tir", the star was portrayed as the arrow itself in later Persian culture.
Sirius is mentioned in Surah, An-Najm ("The Star"), of the Qur'an, where it is given the name الشِّعْرَى (transliteration: aš-ši‘rā or ash-shira; the leader). The verse is: "وأنَّهُ هُوَ رَبُّ الشِّعْرَى", "That He is the Lord of Sirius (the Mighty Star)." (An-Najm:49) Ibn Kathir said in his commentary "Ibn 'Abbas, Mujahid, Qatada and Ibn Zayd said about Ash-Shi`ra that it is the bright star, named Mirzam Al-Jawza' (Sirius), which a group of Arabs used to worship." The alternate name Aschere, used by Johann Bayer, is derived from this.
In Theosophy, it is believed the Seven Stars of the Pleiades transmit the spiritual energy of the Seven Rays from the Galactic Logos to the Seven Stars of the Great Bear, then to Sirius. From there is it sent via the Sun to the god of Earth (Sanat Kumara), and finally through the seven Masters of the Seven Rays to the human race.
The Dogon people are an ethnic group in Mali, West Africa, reported to have traditional astronomical knowledge about Sirius that would normally be considered impossible without the use of telescopes. According to Marcel Griaule's books Conversations with Ogotemmêli and The Pale Fox they knew about the fifty-year orbital period of Sirius and its companion prior to western astronomers. They also refer to a third star accompanying Sirius A and B. Robert Temple's 1976 book The Sirius Mystery, credits them with knowledge of the four Galilean moons of Jupiter and the rings of Saturn. This has been the subject of controversy and speculation.
In particular, Noah Brosch explained in his book Sirius Matters that the cultural transfer of relatively modern astronomical information could have taken place in 1893, when a French expedition arrived in Central West Africa to observe the total eclipse on April 16.
In the religion of the Serer people of Senegal, The Gambia and Mauritania, Sirius is called Yoonir from the Serer language (and some of the Cangin language speakers, who are all ethnically Serers). The star Sirius is one of the most important and sacred stars in Serer religious cosmology and symbolism. The Serer high priests and priestesses, (Saltigues, the hereditary "rain priests") chart Yoonir in order to forecast rain fall and enable Serer farmers to start planting seeds. In Serer religious cosmology, it is the symbol of the universe.
Sirius is a frequent subject of science fiction, and has been the subject of poetry. Dante and John Milton reference the star, while Tennyson's poem The Princess wonderfully describes the star's scintillation:
..the fiery Sirius alters hue
And bickers into red and emerald.
The Grateful Dead mention the dog star in the song "Lost Sailor".
Sirius is featured on the coat of arms of Macquarie University, and is the name of its alumnae journal. The name of the North American satellite radio company, Satellite CD Radio, Inc., was changed to Sirius Satellite Radio in November 1999, being named after "the brightest star in the night sky". Composer Karlheinz Stockhausen, who wrote a piece called Sirius, has been claimed to have said on several occasions that he came from a planet in the Sirius system. To Stockhausen, Sirius stood for 'the place where music is the highest of vibrations' and where music had been developed in the most perfect way. Astronomer Noah Brosch has speculated that the name of the character Sirius Black from the Harry Potter stories, who owns a unique ability to transform into a black dog, might have been inspired by "Sirius B".
Seven ships of Great Britain's Royal Navy have been called HMS Sirius since the 18th century, with the first being the flagship of the First Fleet to Australia in 1788. The Royal Australian Navy subsequently named a vessel HMAS Sirius in honor of the flagship. American vessels include the USNS Sirius as well as a monoplane model—the Lockheed Sirius, the first of which was flown by Charles Lindbergh. The name was also adopted by Mitsubishi Motors for the Mitsubishi Sirius engine in 1980.
- Astrometric data, mirrored by SIMBAD from the Hipparcos catalogue, pertains to the center of mass of the Sirius system. See § 2.3.4, Volume 1, The Hipparcos and Tycho Catalogues, European Space Agency, 1997, and the entry for Sirius in the Hipparcos catalogue (CDS ID I/239.)
- For apparent magnitude m and parallax π, the absolute magnitude Mv of Sirius A is given by:
- Bolometric luminosity of Sirius B calculated from L=4πR2σTeff4. (This simplifies to Ls=(Rs)^2*(Ts)^4, where Ls, Rs and Ts are Luminosity, Radius and Temperature all relative to solar values) See: Tayler, Roger John (1994). The Stars: Their Structure and Evolution. Cambridge University Press. p. 16. ISBN 0-521-45885-4.
- Coincides with parallax by Perryman et al. (1997).
- Weighted parallax based on parallaxes from van Altena et al. (1995) and van Leeuwen (2007).
- Two full 50.09-year orbits following the periastron epoch of 1894.13 gives a date of 1994.31.
- semi-major axis in AU = semimajor axis in seconds / parallax = 7.56″ / 0.37921 = 19.8 A.U.; as the eccentricity is 0.6, the distance fluctuates between 40% and 160% of that, roughly from 8 AU to 32 AU
- "Sirius". Dictionary.com Unabridged (v 1.1). Random House, Inc. Retrieved 2008-04-06.
- Database entry for Sirius A, SIMBAD. Accessed online October 20, 2007.
- McCook, G. P.; Sion, E. M. "Entry for WD 0642-166". A Catalogue of Spectroscopically Identified White Dwarfs (August 2006 version). CDS. ID III/235A.)
- Hoffleit, D.; Warren, Jr., W. H. (1991). "Entry for HR 2491". Bright Star Catalogue, 5th Revised Ed. (Preliminary Version). CDS. ID V/50.
- van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357
- van den Bos, W. H. (1960). "The Orbit of Sirius". Journal des Observateurs 43: 145–151. Bibcode:1960JO.....43..145V.
- Liebert, J.; Young, P. A.; Arnett, D.; Holberg, J. B.; Williams, K. A. (2005). "The Age and Progenitor Mass of Sirius B". The Astrophysical Journal 630 (1): L69–L72. arXiv:astro-ph/0507523. Bibcode:2005ApJ...630L..69L. doi:10.1086/462419.
- Adelman, Saul J. (July 8–13, 2004). "The Physical Properties of normal A stars". Proceedings of the International Astronomical Union. Poprad, Slovakia: Cambridge University Press. pp. 1–11. Bibcode:2004IAUS..224....1A.
- Qiu, H. M.; Zhao, G.; Chen, Y. Q.; Li, Z. W. (2001). "The Abundance Patterns of Sirius and Vega". The Astrophysical Journal 548 (2): 953–965. Bibcode:2001ApJ...548..953Q. doi:10.1086/319000.
- Royer, F.; Gerbaldi, M.; Faraggiana, R.; Gómez, A. E. (2002). "Rotational velocities of A-type stars. I. Measurement of v sin i in the southern hemisphere". Astronomy and Astrophysics 381 (1): 105–121. arXiv:astro-ph/0110490. Bibcode:2002A&A...381..105R. doi:10.1051/0004-6361:20011422.
- Holberg, J. B.; Barstow, M. A.; Bruhweiler, F. C.; Cruise, A. M.; Penny, A. J. (1998). "Sirius B: A New, More Accurate View". The Astrophysical Journal 497 (2): 935–942. Bibcode:1998ApJ...497..935H. doi:10.1086/305489.
- Hinckley, Richard Allen (1899). Star-names and Their Meanings. New York: G. E. Stechert. pp. 117–25.
- Gingerich, O. (1987). "Zoomorphic Astrolabes and the Introduction of Arabic Star Names into Europe". Annals of the New York Academy of Sciences 500: 89–104. Bibcode:1987NYASA.500...89G. doi:10.1111/j.1749-6632.1987.tb37197.x.
- Singh, Nagendra Kumar (2002). Encyclopaedia of Hinduism, A Continuing Series. Anmol Publications PVT. LTD. p. 794. ISBN 81-7488-168-9.
- Spahn, Mark; Hadamitzky, Wolfgang; Fujie-Winter, Kimiko (1996). The Kanji dictionary. Tuttle language library (Tuttle Publishing). p. 724. ISBN 0-8048-2058-9.
- Database entry for Sirius B, SIMBAD. Accessed on line October 23, 2007.
- van Altena, W. F.; Lee, J. T.; Hoffleit, E. D. (1995). The general catalogue of trigonometric parallaxes (4th ed.). Yale University Observatory. (CDS) ID I/238A.
- Schaaf, Fred (2008). The Brightest Stars. Hoboken, New Jersey: John Wiley & Sons. p. 94. ISBN 0-471-70410-5. Retrieved 2010-07-23.
- Perryman, M. A. C.; Lindegren, L.; Kovalevsky, J. et al. (July 1997), "The Hipparcos Catalogue", Astronomy and Astrophysics 323: L49–L52, Bibcode:1997A&A...323L..49P
- Perryman, Michael (2010), The Making of History's Greatest Star Map, Heidelberg: Springer-Verlag, doi:10.1007/978-3-642-11602-5
- Sky and Telescope, April 1998 (p60), based on computations from Hipparcos data.
- Wendorf, Fred; Schild, Romuald (2001). Holocene Settlement of the Egyptian Sahara: Volume 1, The Archaeology of Nabta Plain (GOOGLE BOOK SEARCH PREVIEW). Springer. p. 500. ISBN 0-306-46612-0. Retrieved 2008-05-16.
- Holberg 2007, pp. 4–5
- Holberg 2007, p. 19
- Holberg 2007, p. 20
- Holberg 2007, pp. 16–17
- Ovid. Fasti IV, lines 901–942.
- Holberg 2007, p. 32
- Holberg 2007, p. 25
- Holberg 2007, pp. 25–26
- Henry, Teuira (1907). "Tahitian Astronomy: Birth of Heavenly Bodies". The Journal of the Polynesian Society 16 (2): 101–04. JSTOR 20700813.
- Makemson 1941, p. 198.
- Makemson 1941, p. 280.
- Makemson 1941, p. 218.
- Makemson 1941, p. 207.
- Makemson 1941, p. 219.
- Makemson 1941, p. 209.
- Makemson 1941, p. 214.
- Makemson 1941, p. 265.
- Makemson 1941, p. 257.
- Makemson 1941, p. 266.
- Hamacher, Duane W.; Frew, David J. (2010). "An Aboriginal Australian Record of the Great Eruption of Eta Carinae" (PDF). Journal of Astronomical History & Heritage 13 (3): 220–34.
- Aitken, R. G. (1942). "Edmund Halley and Stellar Proper Motions". Astronomical Society of the Pacific Leaflets 4: 103–112. Bibcode:1942ASPL....4..103A.
- Holberg 2007, pp. 41–42
- Daintith, John; Mitchell, Sarah; Tootill, Elizabeth; Gjertsen, D. (1994). Biographical Encyclopedia of Scientists. CRC Press. p. 442. ISBN 0-7503-0287-9.
- Huggins, W. (1868). "Further observations on the spectra of some of the stars and nebulae, with an attempt to determine therefrom whether these bodies are moving towards or from the Earth, also observations on the spectra of the Sun and of Comet II". Philosophical Transactions of the Royal Society of London 158 (0): 529–564. Bibcode:1868RSPT..158..529H. doi:10.1098/rstl.1868.0022.
- Maskelyne, Nevil (1761). "A Proposal for Discovering the Annual Parallax of Sirius; by the Rev. Nevil Maskelyne, a. M. Fellow of Trinity College, Cambridge, and F. R. S.". Philosophical Transactions of the Royal Society 51 (2): 889–895. Bibcode:1759RSPT...51..889M. doi:10.1098/rstl.1759.0080. Google Books id: zBdWAAAAYAAJ — page 889
- Henderson, T. (1840). "On the Parallax of Sirius". Monthly Notices of the Royal Astronomical Society 11: 239. Bibcode:1840MmRAS..11..239H.
- Woolley R.; Epps E. A.; Penston M. J.; Pocock S. B. (1970). "Woolley 244". Catalogue of stars within 25 parsecs of the Sun. Retrieved 2014-06-05.
- Gliese, W. and Jahreiß, H. (1991). "Gl 244". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 2014-06-05.
- Van Altena W. F., Lee J. T., Hoffleit E. D. (1995). "GCTP 1577". The General Catalogue of Trigonometric Stellar Parallaxes (Fourth ed.). Retrieved 2014-06-05.
- Perryman et al. (1997). "HIP 32349". The Hipparcos and Tycho Catalogues. Retrieved 2014-06-05.
- Perryman et al. (1997). "HIP 32349". The Hipparcos and Tycho Catalogues. Retrieved 2014-06-05.
- van Leeuwen F. (2007). "HIP 32349". Validation of the new Hipparcos reduction. Retrieved 2014-06-05.
- "RECONS TOP100". THE ONE HUNDRED NEAREST STAR SYSTEMS brought to you by RECONS (Research Consortium On Nearby Stars). 2012. Retrieved 2014-06-05.
- Bessel, F. W.; communicated by Herschel, J. F. W. (December 1844). "On the Variations of the Proper Motions of Procyon and Sirius". Monthly Notices of the Royal Astronomical Society 6: 136–141. Bibcode:1844MNRAS...6..136.. doi:10.1093/mnras/6.11.136a.
- Flammarion, Camille (August 1877). "The Companion of Sirius". The Astronomical Register 15 (176): 186–189. Bibcode:1877AReg...15..186F.
- Craig, John; Gravatt, William; Slater, Thomas; Rennie, George. "The Craig Telescope". craig-telescope.co.uk. Retrieved 2011-03-01.
- Appletons' annual cyclopaedia and register of important events of the year: 1862. New York: D. Appleton & Company. 1863. p. 176.
- Benest, D.; Duvent, J. L.; Duvent (July 1995). "Is Sirius a triple star?". Astronomy and Astrophysics 299: 621–628. Bibcode:1995A&A...299..621B. – For the instability of an orbit around Sirius B, see § 3.2.
- Bonnet-Bidaud, J. M.; Pantin, E. (October 2008). "ADONIS high contrast infrared imaging of Sirius-B". Astronomy and Astrophysics 489 (2): 651–655. arXiv:0809.4871. Bibcode:2008A&A...489..651B. doi:10.1051/0004-6361:20078937.
- Adams, W. S. (December 1915). "The Spectrum of the Companion of Sirius". Publications of the Astronomical Society of the Pacific 27 (161): 236–237. Bibcode:1915PASP...27..236A. doi:10.1086/122440.
- Holberg, J. B. (2005). "How Degenerate Stars Came to be Known as White Dwarfs". Bulletin of the American Astronomical Society 37 (2): 1503. Bibcode:2005AAS...20720501H.
- Brown, R. Hanbury; Twiss, R. Q. (1958). "Interferometry of the Intensity Fluctuations in Light. IV. A Test of an Intensity Interferometer on Sirius A". Proceedings of the Royal Society of London 248 (1253): 222–237. Bibcode:1958RSPSA.248..222B. doi:10.1098/rspa.1958.0240.
- Brown, Dwayne; Weaver, Donna (2005-12-13). "Astronomers Use Hubble to "Weigh" Dog Star's Companion". NASA. Retrieved 2007-10-13.
- McGourty, Christine (2005-12-14). "Hubble finds mass of white dwarf". BBC News. Retrieved 2007-10-13.
- Bond, Peter (2005-12-14). "Astronomers Use Hubble to 'Weigh' Dog Star's Companion". Royal Astronomical Society. Retrieved 2015-03-10.
- Barstow, M. A.; Bond, Howard E.; Holberg, J. B.; Burleigh, M. R.; Hubeny, I.; Koester, D. (2005). "Hubble Space Telescope spectroscopy of the Balmer lines in Sirius B". Monthly Notices of the Royal Astronomical Society 362 (4): 1134–1142. arXiv:astro-ph/0506600. Bibcode:2005MNRAS.362.1134B. doi:10.1111/j.1365-2966.2005.09359.x.
- Holberg 2007, p. 157
- Ceragioli, R. C. (1995). "The Debate Concerning 'Red' Sirius". Journal for the History of Astronomy 26 (3): 187–226. Bibcode:1995JHA....26..187C.
- Holberg 2007, p. 158
- Holberg 2007, p. 161
- Holberg 2007, p. 162
- Whittet, D. C. B. (1999). "A physical interpretation of the 'red Sirius' anomaly". Monthly Notices of the Royal Astronomical Society 310 (2): 355–359. Bibcode:1999MNRAS.310..355W. doi:10.1046/j.1365-8711.1999.02975.x.
- Holberg 2007, p. 163
- 江晓原 (1992). 中国古籍中天狼星颜色之记载. Ť�文学报 (in Chinese) 33 (4).
- Jiang, Xiao-Yuan (April 1993). "The colour of Sirius as recorded in ancient Chinese texts". Chinese Astronomy and Astrophysics 17 (2): 223–228. Bibcode:1993ChA&A..17..223J. doi:10.1016/0275-1062(93)90073-X.
- Schlosser, W.; Bergmann, W. (November 1985). "An early-medieval account on the red colour of Sirius and its astrophysical implications". Nature 318 (318): 45–46. Bibcode:1985Natur.318...45S. doi:10.1038/318045a0.
- McCluskey, S. C. (January 1987). "The colour of Sirius in the sixth century". Nature 318 (325): 87. Bibcode:1987Natur.325...87M. doi:10.1038/325087a0.
- van Gent, R. H. (January 1987). "The colour of Sirius in the sixth century". Nature 318 (325): 87–89. Bibcode:1987Natur.325...87V. doi:10.1038/325087b0.
- Kuchner, Marc J.; Brown, Michael E. (2000). "A Search for Exozodiacal Dust and Faint Companions Near Sirius, Procyon, and Altair with the NICMOS Coronagraph". Publications of the Astronomical Society of the Pacific 112 (772): 827–832. arXiv:astro-ph/0002043. Bibcode:2000PASP..112..827K. doi:10.1086/316581.
- "The Dog Star, Sirius, and its Tiny Companion". Hubble News Desk. 2005-12-13. Retrieved 2006-08-04.
- Holberg 2007, p. xi
- Espenak, Fred. "Mars Ephemeris". Twelve Year Planetary Ephemeris: 1995–2006, NASA Reference Publication 1349.
- Holberg 2007, p. 82
- Darling, David. "Winter Triangle". The Internet Encyclopedia of Science. Retrieved 2007-10-20.
- "Stories from the Stars". Stargazers Astronomy Shop. 2000. Retrieved 2008-12-17.
- Henshaw, C. (1984). "On the Visibility of Sirius in Daylight". Journal of the British Astronomical Association 94 (5): 221–222. Bibcode:1984JBAA...94..221H.
- Mullaney, James (March 2008). "Orion's Splendid Double Stars: Pretty Doubles in Orion's Vicinity". Sky & Telescope. Retrieved 2008-02-01.
- Henry, Todd J. (2006-07-01). "The One Hundred Nearest Star Systems". RECONS. Retrieved 2006-08-04.
- "The Brightest Stars". Royal Astronomical Society of New Zealand. Retrieved 2007-12-14.
- "Sirius 2". SolStation. Retrieved 2006-08-04.
- Angrum, Andrea (2005-08-25). "Interstellar Mission". NASA/JPL. Retrieved 2007-05-07.
- Holberg 2007, p. 214
- Backman, D. E. (June 30 – July 11, 1986). "IRAS observations of nearby main sequence stars and modeling of excess infrared emission". In Gillett, F. C.; Low, F. J. Proceedings, 6th Topical Meetings and Workshop on Cosmic Dust and Space Debris. Toulouse, France: COSPAR and IAF. Bibcode:1986AdSpR...6...43B. ISSN 0273-1177.
- Brosch 2008, p. 126
- Bragança, Pedro (2003-07-15). "The 10 Brightest Stars". SPACE.com. Archived from the original on 2009-06-16. Retrieved 2006-08-04.
- Kervella, P.; Thevenin, F.; Morel, P.; Borde, P.; Di Folco, E. (2003). "The interferometric diameter and internal structure of Sirius A". Astronomy and Astrophysics 407 (2): 681–688. arXiv:astro-ph/0306604. Bibcode:2003A&A...408..681K. doi:10.1051/0004-6361:20030994.
- Aufdenberg, J.P.; Ridgway, S.T. et al. (2006). "First results from the CHARA Array: VII. Long-Baseline Interferometric Measurements of Vega Consistent with a Pole-On, Rapidly Rotating Star?" (PDF). Astrophysical Journal 645 (1): 664–675. arXiv:astro-ph/0603327. Bibcode:2006ApJ...645..664A. doi:10.1086/504149. Retrieved 2007-11-09.
- Petit, P. et al. (August 2011). "Detection of a weak surface magnetic field on Sirius A: are all tepid stars magnetic?". Astronomy and Astrophysics 532: L13. arXiv:1106.5363. Bibcode:2011A&A...532L..13P. doi:10.1051/0004-6361/201117573.
- Aurière, M. et al. (November 2010). "No detection of large-scale magnetic fields at the surfaces of Am and HgMn stars". Astronomy and Astrophysics 523: A40. arXiv:1008.3086. Bibcode:2010A&A...523A..40A. doi:10.1051/0004-6361/201014848.
- "Astronomers Use Hubble to "Weigh" Dog Star's Companion". University of Leicester. 2005-12-01. Retrieved 2009-12-13.
- Imamura, James N. (1995-10-02). "Cooling of White Dwarfs". University of Oregon. Archived from the original on December 15, 2006. Retrieved 2007-01-03.
- Siess, Lionel (2000). "Computation of Isochrones". Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles. Retrieved 2007-03-24.
- Palla, Francesco (May 16–20, 2005). "Stellar evolution before the ZAMS". Proceedings of the international Astronomical Union 227. Italy: Cambridge University Press. pp. 196–205. Bibcode:976IAUS...73...75P.
- Koester, D.; Chanmugam, G. (1990). "Physics of white dwarf stars". Reports on Progress in Physics 53 (7): 837–915. Bibcode:1990RPPh...53..837K. doi:10.1088/0034-4885/53/7/001.
- Holberg, J. B.; Barstow, M. A.; Burleigh, M. R.; Kruk, J. W.; Hubeny, I.; Koester, D. (2004). "FUSE observations of Sirius B". Bulletin of the American Astronomical Society 36: 1514. Bibcode:2004AAS...20510303H.
- Frommert, Hartmut; Kronberg, Christine (April 26, 2003). "The Ursa Major Moving Cluster, Collinder 285". SEDS. Archived from the original on 2007-12-20. Retrieved 2007-11-22.
- King, Jeremy R.; Villarreal, Adam R.; Soderblom, David R.; Gulliver, Austin F.; Adelman, Saul J. (2003). "Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group". Astronomical Journal 125 (4): 1980–2017. Bibcode:2003AJ....125.1980K. doi:10.1086/368241.
- Croswell, Ken (July 27, 2005). "The life and times of Sirius B". Astronomy, online. Retrieved 2007-10-19.
- Eggen, Olin J. (1992). "The Sirius supercluster in the FK5". Astronomical Journal 104 (4): 1493–1504. Bibcode:1992AJ....104.1493E. doi:10.1086/116334.
- Olano, C. A. (2001). "The Origin of the Local System of Gas and Stars". The Astronomical Journal 121 (1): 295–308. Bibcode:2001AJ....121..295O. doi:10.1086/318011.
- Liddell, Henry G.; Scott, Robert (1980). Greek-English Lexicon (Abridged ed.). Oxford: Oxford University Press. ISBN 0-19-910207-4.
- Holberg 2007, pp. 15–16
- Brosch 2008, p. 21
- Kak, Subhash. "Indic ideas in the Greco-Roman world". IndiaStar Review of Books. Retrieved 2010-07-23.
- "Shri Shri Shiva Mahadeva".
- "Makarajyothi is a star: senior Thantri". The Hindu. 2011-01-24. Retrieved 2014-01-09.
- Rydberg, Viktor (1889). Rasmus Björn Anderson, ed. Teutonic mythology 1. S. Sonnenschein & co.
- Tyson, Donald; Freake, James (1993). Three Books of Occult Philosophy. Llewellyn Worldwide. ISBN 0-87542-832-0.
- Agrippa, Heinrich Cornelius (1533). De Occulta Philosophia. ISBN 90-04-09421-0.
- Homer (1997). Iliad. Trans. Stanley Lombardo. Indianapolis: Hackett. ISBN 978-0-87220-352-5. 22.33–37.
- Doostkhah, Jalil (1996). Avesta. Kohantarin Sorōdhāye Irāniān. Tehran: Morvarid Publications. ISBN 964-6026-17-6.
- West, E. W. (1895–1910). Pahlavi Texts. Routledge Curzon, 2004. ISBN 0-7007-1544-4.
- Razi, Hashem (2002). Encyclopaedia of Ancient Iran. Tehran: Sokhan Publications. ISBN 964-372-027-6.
- Ferdowsi, A. Shahnameh e Ferdowsi. Bank Melli Iran Publications, 2003. ISBN 964-93135-3-2.
- Holberg 2007, p. 22
- Holberg 2007, p. 23
- Holberg 2007, p. 24
- Staff (2007). "Sirius". Britannica Online Encyclopedia. Retrieved 2007-09-10.
- "An-Najm (The Star), Surah 53". Translations of the Qur'an. University of Southern California, Center for Muslim-Jewish Engagement. 2007. Retrieved 2009-08-08.
- "Tafsir Ibn Kathir". 2012-07-09.
- Baker, Douglas (1977). The Seven Rays: Key to the Mysteries. Wellingborough, Herts.: Aquarian Press. ISBN 0-87728-377-X.
- Gravrand, Henry, "La civilisation sereer : Pangool", vol. 2, Les Nouvelles Editions Africaines du Sénégal, (1990) pp 20-21, 149-155, ISBN 2-7236-1055-1
- Clémentine Faïk-Nzuji Madiya, Canadian Museum of Civilization, Canadian Centre for Folk Culture Studies, International Centre for African Language, Literature and Tradition (Louvain, Belgium). ISBN 0-660-15965-1. pp 5, 27, 115
- Galvan, Dennis Charles, The State Must be our Master of Fire : How Peasants Craft Culturally Sustainable Development in Senegal, Berkeley, University of California Press, (2004), pp 86-135, ISBN 978-0-520-23591-5.
- The editors of Asimov's Science Fiction and Analog (1993). Writing Science Fiction & Fantasy. St. Martin's Griffin. p. 108. ISBN 978-0-312-08926-9.
- Brosch 2008, p. 33
- LacusCurtius • Allen's Star Names — Canis Major
- "About Macquarie University—Naming of the University". Macquarie University official website. Macquarie University. 2007. Retrieved 2007-12-27.
- "Sirius Satellite Radio, Inc. – Company Profile, Information, Business Description, History, Background Information on Sirius Satellite Radio, Inc". Net Industries, LLC. Retrieved 2008-01-22.
- McEnery, Paul (2001-01-16). "Karlheinz Stockhausen". Salon.com.
- Tom Service (2005-10-13). "Beam Me up, Stocky". The Guardian.
- Michael Kurtz, Stockhausen. Eine Biografie. Kassel, Bärenreiter Verlag, 1988: p. 271
- Duarte, Paulo Araújo. "Astronomia na Bandeira Brasileira". Universidade Federal de Santa Catarina. Retrieved 2009-07-09.
- Henderson, G.; Stanbury, M. (1988). The Sirius: Past and Present. Sydney: Collins. p. 38. ISBN 0-7322-2447-0.
- "HMAS Sirius". Royal Australian Navy. Retrieved 2008-09-13.
- van der Linden, F. R. (2000). "Lockheed 8 Sirius". National Air and Space Museum. Smithsonian Institution. Archived from the original on 2008-01-05. Retrieved 2008-01-26.
- "Mitsubishi Motors history". Mitsubishi Motors – South Africa Official Website. Mercedes Benz. 2007. Archived from the original on 2007-12-30. Retrieved 2008-01-27.
- Brosch, Noah (2008). Sirius Matters. Springer. ISBN 1-4020-8318-1.
- Holberg, J.B. (2007). Sirius: Brightest Diamond in the Night Sky. Chichester, UK: Praxis Publishing. ISBN 0-387-48941-X.
- Makemson, Maud Worcester (1941), The Morning Star Rises: An Account of Polynesian Astronomy, Yale University Press
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- Barker, Tho.; Stukeley, W. (1760). "Remarks on the Mutations of the Stars". Philosophical Transactions 51 (0): 498–504. doi:10.1098/rstl.1759.0049. JSTOR 105393.